Galaxy formation with warm dark matter
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Galaxy formation with warm dark matter. Mark Lovell Adrian Jenkins, Carlos Frenk , Vince Eke, Tom Theuns , Liang Gao , Shi Shao, Simon White, Alexey Boyarsky , Oleg Ruchayskiy …. Ripples in the Cosmos 22/07/2013. Outline. WDM reminder (see Carlos’ talk)

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Galaxy formation with warm dark matter

Galaxy formation with warm dark matter

Mark Lovell

Adrian Jenkins, Carlos Frenk, Vince Eke, Tom Theuns, Liang Gao, Shi Shao, Simon White, Alexey Boyarsky, Oleg Ruchayskiy…

Ripples in the Cosmos 22/07/2013


Outline
Outline

  • WDM reminder (see Carlos’ talk)

  • How does subhalo structure change with WDM particle mass?

  • Effect of WDM on reionisation?


N msm
nMSM

  • Neutrino Minimal Standard Model (nMSM) conceived to explain neutrino masses (Asaka & Shaposhnikov, 2005).

  • Adds three sterile neutrinos to the SM. The lightest of these would be a dark matter candidate.

  • Large velocities at early times => WDM / CWDM

U

C

T

g

D

S

B

g

e

m

t

W

ne

nm

nt

Z

H

N1

N2

N3


WDM

  • Phase space limit (small cores ~pc)

  • Free-streaming

  • Low mass substructures suppressed.

  • Later formation times

  • Concentrations lower

  • Reionisation delayed

Lovell et al. 2012


Subhalo structure
Subhalo structure


Simulation suite vital statistics
Simulation Suite – Vital Statistics

  • 5 resimulations of the Aquarius Aq-A halo: 4WDM models + CDM, WMAP7 cosmology

  • Dark matter simulation particle mass 1.5x104Msun

  • WDM particle masses mp=1.4keV, 1.6keV, 2.0keV, 2.3keV (thermal relics)

  • PWDM/PCDM = (1+(ak)n)-10/n [n=1]

  • a=a[mp]


PWDM/PCDM = (1+(ak)n)-10/n [n=1]

(Bode et al. 2001)

m1.4

m1.6

m2.0

m2.3

CDM

Lovell et al. (in prep.)


z=3


M sub v max
Msub - Vmax

Lovell et al. (in prep.)


V max r max concentration
Vmax – rmax[concentration]

WMAP7

WMAP1

Lovell et al. (in prep.)


Nfw vs einasto
NFW vsEinasto

Lovell et al. (in prep.)


Density profiles 1
Density Profiles (1)

Lovell et al. (in prep.)


Density profiles 2
Density Profiles (2)

Lovell et al. (in prep.)


V circ profiles
Vcirc profiles


Central densities
Central Densities

# Too Big to Fail:

CDM: 6

m2.3: 4

m2.0: 3

m1.6: 3

m1.4: 1

Field Haloes

Subhaloes

No Problem for WDM



Simulations
Simulations

No feedback

Feedback enabled

  • Aq-A4 halo

  • SPH – Gadget3 code

  • CDM/WDM vs. Supernova feedback/no feedback

  • Salpeter IMF

  • Multiphase ISM

  • Primordial cooling tables

  • Decoupled winds (Springel&Hernquist 2003)

CN

CW

CDM

WN

WW

WDM (1.4keV)




Reionising the local universe
Reionising the (Local) Universe…

Preliminary

Warning!!

Uber-simple model!



Conclusions
Conclusions

  • Exciting WDM / CWDM models motivated by nMSM

  • Subhalo structure

    • Vmaxes, central densities lower with progressively warmer models at a given mass – alleviates ‘too big too fail’ problem. Cosmology also plays a role.

  • Reionisation

    • WDM models produce enough photons to reionise each hydrogen atom, subgrid model important.


Mass functions
Mass functions

Lovell et al. (in prep.)


Since you asked
Since you asked…

Lovell et al. (in prep.)


S

S

Lovell et al. (in prep)


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